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Dan Hooper - Fermilab/University of Chicago Community Summer Study (Snomass 2013)

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Dan Hooper - Fermilab/University of Chicago Community Summer Study (Snomass 2013) Dan Hooper - Fermilab/University of Chicago Community Summer Study (Snomass 2013) On behalf of the CF4 Working Group (Manoj Kaplinghat, Konstantin Matchev, DH) The Dark Matter Discovery Age In a sense, we have already discovered dark matter Observations of galaxy dynamics, galaxy clusters, large scale structure, the cosmic microwave background, light element abundances, etc. collectively provide an overwhelming body of evidence in favor of the conclusion that most of the matter in our Universe consists of (relatively) cold and collisionless particles Despite considerable effort, no viable alternatives to this conclusion have been proposed But we have not yet identified the nature of the particle(s) that make up the dark matter No particles contained in the standard model are viable dark matter candidates – dark matter is new physics The Dark Matter Discovery Age In a sense, we have already discovered dark matter Observations of galaxy dynamics, galaxy clusters, large scale structure, the cosmic microwave background, light element abundances, etc. collectively provide an overwhelming body of evidence in favor of the conclusion that most of the matter in our Universe consists of (relatively) cold and collisionless particles Despite considerable effort, no viable alternatives to this conclusion have been proposed But we have not yet identified the nature of the particle(s) that make up the dark matter No particles contained in the standard model are viable dark matter candidates – dark matter is new physics After decades of experimental progress, we are currently in a position in which many or most of the best motivated dark matter candidates are within reach of near future experiments – The successful detection of dark matter particles within the next decade seems likely SLAC 5/25/13 18:39 Cryogenic Solid State CDMS/SuperCDMS EDELWEISS/CRESST/EURECA CoGeNT/C4 TEXONO/CDEX Liquid Xenon LUX/LZ XENON PandaX XMASS Liquid Argon ArDM Darkside DEAP CLEAN Crystal and Annual Modulation DAMA/LIBRA KIMS ELEGANT ANAIS SLAC 5/25/13 18:39 CINDMS Princeton NaI WIMP Direct Detection CensusDM-Ice Cryogenic Solid State CDMS/SuperCDMS Threshold Detectors EDELWEISS/CRESST/EURECA Technology Description 1. Experiment Status, Target Mass CoGeNT/C4 PICASSO TEXONO/CDEX SIMPLE 2. Fiducial target mass COUPP 3. Backgrounds after passive and Liquid Xenon LUX/LZ Directional Detection active shielding. XENON DRIFT PandaX Newage 4. Detector Discrimination XMASS DMTPC MIMAC 5. Energy Threshold D3 Liquid Argon 6. Sensitivity versus WIMP mass ArDM New Ideas Darkside DEAP DAMIC 7. Experimental Challenges CLEAN Liquid helium-4 Direct Detection NEXT 8. Annual Modulation …'and'this'progress'is'expected'to'con,nue.'Nuclear emulsions (Naka, Japan) Crystal and Annual Modulation DNA & Nano-explosions (Drukier/Cantor) 9. Unique Over Capabilities the past dozen years, DAMA/LIBRA 2 KIMS Evolution of the sSI for a 50 GeV c WIMP constraints from direct detection -39 THE QUESTIONS 10. Determining WIMP properties ELEGANT 10 ANAIS ‡ experiments have improved withCINDMS ‡ ‡ -41 and astrophysical parameters Princeton NaI D 10 ‡ ê 2 Ê 1. Experiment Status and Target Mass a Moore’s-law like behavior DM-Ice ÊÊÊ cm Ê Cryogenic Detectors @ Ú SI Is yourÊ experiment currently operating, and with what total target mass? -43 Ê Crystals (a factor of 2 every 15 months) s 10 Ú ‡ If not, whenÚÊ doÚÊ you expect to operate, and with what total target mass? Threshold Detectors What total targetÚ mass do you expect ÏtoLiquid haveArgon operating 10 years from now? http://www.snowmass2013.org/ tiki- -45 ÚÁ Ì Ú Liquid Xenon Nucleon 10 Ì Technology Description- 2. Fiducial targetÛ massÁ PICASSO ıÌ Ù Threshold Detectors index.php?page =SLAC SIMPLE WIMP Û 10-47 Ì COUPP http://www.snowmass2013.org/tiki-index.php?page=SLAC Page 3 of 5 Û 10-49 1990 2000 2010 2020 Directional Detection Year DRIFT 29 July 2013 NewageCosmic Frontier Intro D.'McKinsey''''''''Direct'Detec,on' 11 DMTPC MIMAC D3 New Ideas DAMIC Liquid helium-4 NEXT Nuclear emulsions (Naka, Japan) DNA & Nano-explosions (Drukier/Cantor) THE QUESTIONS 1. Experiment Status and Target Mass Is your experiment currently operating, and with what total target mass? If not, when do you expect to operate, and with what total target mass? What total target mass do you expect to have operating 10 years from now? 2. Fiducial target mass http://www.snowmass2013.org/tiki-index.php?page=SLAC Page 3 of 5 SLAC 5/25/13 18:39 Cryogenic Solid State CDMS/SuperCDMS EDELWEISS/CRESST/EURECA CoGeNT/C4 TEXONO/CDEX Liquid Xenon LUX/LZ XENON PandaX XMASS Liquid Argon ArDM Darkside DEAP CLEAN Crystal and Annual Modulation DAMA/LIBRA KIMS ELEGANT ANAIS SLAC 5/25/13 18:39 CINDMS Princeton NaI WIMP Direct Detection CensusDM-Ice Cryogenic Solid State CDMS/SuperCDMS Threshold Detectors EDELWEISS/CRESST/EURECA Technology Description 1. Experiment Status, Target Mass CoGeNT/C4 PICASSO TEXONO/CDEX SIMPLE 2. Fiducial target mass COUPP 3. Backgrounds after passive and Liquid Xenon LUX/LZ Directional Detection active shielding. XENON DRIFT PandaX Newage 4. Detector Discrimination XMASS DMTPC MIMAC 5. Energy Threshold D3 Liquid Argon 6. Sensitivity versus WIMP mass ArDM New Ideas Darkside DEAP DAMIC 7. Experimental Challenges CLEAN Liquid helium-4 Direct Detection NEXT 8. Annual Modulation Z-mediated…'and'this'progress'is'expected'to'con,nue.' scatteringNuclear emulsions (Naka, Japan) DNA & Nano-explosions (Drukier/Cantor) Crystal and Annual Modulation (sneutrinos, heavy neutrinos) 9. Unique Over Capabilities the past dozen years, DAMA/LIBRA 2 KIMS Evolution of the sSI for a 50 GeV c WIMP constraints from direct detection -39 THE QUESTIONS 10. Determining WIMP properties ELEGANT 10 ANAIS ‡ experiments have improved withCINDMS ‡ ‡ -41 and astrophysical parameters Princeton NaI D 10 ‡ ê 2 Ê 1. Experiment Status and Target Mass a Moore’s-law like behavior DM-Ice ÊÊÊ cm Ê Cryogenic Detectors @ Ú SI Is yourÊ experiment currently operating, and with what total target mass? -43 Ê Crystals (a factor of 2 every 15 months) s 10 Ú ‡ If not, whenÚÊ doÚÊ you expect to operate, and with what total target mass? Ï Liquid Argon Threshold Detectors What total targetÚ mass do you expect to have operating 10 years from now? http://www.snowmass2013.org/ Some important benchmarkstiki- exist -45 ÚÁ Ì Ú Liquid Xenon Nucleon 10 Ì Technology Description- 2. Fiducial target mass Ûı Á Threshold Detectors index.php?pagealong this =SLACline: PICASSO Ì Ù SIMPLE WIMP Û 10-47 Ì Mid-late 90s: Direct detection COUPP http://www.snowmass2013.org/tiki-index.php?page=SLAC Page 3 of 5 Û experiments excluded the cross 10-49 sections predicted for a WIMP which 1990 2000 2010 2020 Directional Detection Year scatters and annihilates through DRIFT 29 July 2013 Z-exchange NewageCosmic Frontier Intro D.'McKinsey''''''''Direct'Detec,on' 11 DMTPC Now!: Current experiments are MIMAC D3 beginning to test WIMPs which interact Higgs-mediated scattering through Higgs exchange New Ideas (A-funnel, focus point neutralinos) (including many SUSY models) DAMIC Liquid helium-4 DM SM DM DM NEXT Nuclear emulsions (Naka, Japan) DNA & Nano-explosions (Drukier/Cantor) DM SM SM SM THE QUESTIONS 1. Experiment Status and Target Mass Is your experiment currently operating, and with what total target mass? If not, when do you expect to operate, and with what total target mass? What total target mass do you expect to have operating 10 years from now? 2. Fiducial target mass http://www.snowmass2013.org/tiki-index.php?page=SLAC Page 3 of 5 SLAC 5/25/13 18:39 Cryogenic Solid State CDMS/SuperCDMS EDELWEISS/CRESST/EURECA CoGeNT/C4 TEXONO/CDEX Liquid Xenon LUX/LZ XENON PandaX XMASS Liquid Argon ArDM Darkside DEAP CLEAN Crystal and Annual Modulation DAMA/LIBRA KIMS ELEGANT ANAIS SLAC 5/25/13 18:39 CINDMS Princeton NaI WIMP Direct Detection CensusDM-Ice Cryogenic Solid State CDMS/SuperCDMS Threshold Detectors EDELWEISS/CRESST/EURECA Technology Description 1. Experiment Status, Target Mass CoGeNT/C4 PICASSO TEXONO/CDEX SIMPLE 2. Fiducial target mass COUPP 3. Backgrounds after passive and Liquid Xenon LUX/LZ Directional Detection active shielding. XENON DRIFT PandaX Newage 4. Detector Discrimination XMASS DMTPC MIMAC 5. Energy Threshold D3 Liquid Argon 6. Sensitivity versus WIMP mass ArDM New Ideas Darkside DEAP DAMIC 7. Experimental Challenges CLEAN Liquid helium-4 NEXT 8. Annual Modulation …'and'this'progress'is'expected'to'con,nue.'Nuclear emulsions (Naka, Japan) Direct Detection DNA & Nano-explosions (Drukier/Cantor) Crystal and Annual Modulation 9. Unique Capabilities DAMA/LIBRA KIMS 2 If this rate of progress continues without Evolution of the sSI for a 50 GeV c WIMP -39 THE QUESTIONS 10. Determining WIMP properties ELEGANT 10 the observation of a signal for anotherANAIS ‡ CINDMS ‡ ‡ -41 ~5and years, astrophysical the remaining parameters dark matter Princeton NaI D 10 ‡ ê 2 Ê 1. Experiment Status and Target Mass DM-Ice ÊÊÊ cm Ê Cryogenic Detectors models will be severely constrained @ Ú SI Is yourÊ experiment currently operating, and with what total target mass? -43 Ê Crystals s 10 Ú ‡ If not, whenÚÊ doÚÊ you expect to operate, and with what total target mass? Ï Liquid Argon In order for WIMPs to evade detectionThreshold Detectors What total targetÚ mass do you expect to have operating 10 years from now? http://www.snowmass2013.org/tiki- -45 ÚÁ Ì Ú Liquid Xenon Nucleon 10 Ì over this time frame, one must considerTechnology Description - 2. Fiducial target mass Ûı Á Threshold Detectors index.php?page=SLAC PICASSO Ì Ù one or more of the following: SIMPLE WIMP Û 10-47 Ì COUPP http://www.snowmass2013.org/tiki-index.php?page=SLAC Page 3 of 5 WIMPs which couple almost entirely to Û 10-49 leptons or gauge bosons, rather than to 1990 2000 2010 2020 quarks Directional Detection Year DRIFT 29WIMPs July 2013 which annihilate in the early Newage Cosmic Frontier Intro D.'McKinsey''''''''Direct'Detec,on' 11 DMTPC universe through a highly-tuned MIMAC resonance, or through a highly degenerateD3 It is starting to become co-annihilation difficult to hide our best New Ideas motivated dark matter models WIMPs which are light enough to fall below DAMIC from direct detection expts.
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